Chiral gravitational waves produced in a helical magnetogenesis model

Okano, Soh; Fujita, Tomohiro

doi:10.1088/1475-7516/2021/03/026

Cited by 22 publications

(16 citation statements)

References 86 publications

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“…The natural interaction between the axion and dark photon is the so-called Chern-Simons coupling. Such a coupling is very well studied in different contexts like magnetogenesis [22,[47][48][49], inflation [19,50,51], preheating [52] and in axion dark matter models to solve the problem of the overabundance of the axions [6,7]. The Lagrangian density for the dark sector takes the form…”

Section: Introductionmentioning

confidence: 99%

Analytic study of dark photon and gravitational wave production from axion

Salehian

Gorji

Mukohyama

et al. 2021

J. High Energ. Phys.

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Axion-like fields heavier than about 10−27 eV are expected to oscillate in the radiation dominated epoch when the Hubble parameter drops below their mass. Considering the Chern-Simons coupling with a dark gauge boson, large amount of dark photons are produced during a short time interval through tachyonic resonance instability. The produced dark photons then source gravitational tensor modes leading to chiral gravitational waves. Through this process, one can indirectly probe a large parameter space of coupled axion-dark photon models. In this work we first find an analytic expression for the number density of the dark photons produced during the tachyonic resonance regime. Second, by using the saddle point approximation we find an analytic expression for the gravitational wave spectrum in terms of the mass, coupling and misalignment angle. Our analytic results can be used for the observational analysis of these types of scenarios.

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Section: Introductionmentioning

confidence: 99%

Analytic study of dark photon and gravitational wave production from axion

Salehian

Gorji

Mukohyama

et al. 2021

J. High Energ. Phys.

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“…An important extension of the present work is to consider helical magnetogenesis (Turner & Widrow 1988;Garretson et al 1992;Field & Carroll 2000;Anber & Sorbo 2006;Caprini & Sorbo 2014;Adshead et al 2016;Sobol et al 2019). These authors considered an additional chiral symmetry breaking term involving the dual Faraday tensor in the Lagrangian; see also the papers by Sharma et al (2018) and Okano & Fujita (2021). Helical magnetic fields decay more slowly than nonhelical ones and are therefore more likely to survive until present time; see Figure 11 of .…”

Section: Discussionmentioning

confidence: 99%

“…A similar model for chiral magnetic field generation and polarized GWs was recently considered by Sharma et al (2020) and Okano & Fujita (2021). These works are based on earlier work by Fujita et al (2015), Sharma et al (2018), Fujita & Durrer (2019), Durrer et al (2011), andSorbo (2014).…”

Section: Introductionmentioning

confidence: 85%

“…Both analytical considerations (Dolgov et al 2002;Gogoberidze et al 2007) and numerical simulations (Roper Pol et al 2020b) have demonstrated that there can be a direct correspondence between the turbulence spectrum and the resulting GW spectrum. An important additional property of GWs might be their circular polarization, which could be caused by helical turbulence (Kahniashvili et al 2005) or by helical magnetic fields (Namba et al 2016;Niksa et al 2018;Anand et al 2019;Sharma et al 2020;Okano & Fujita 2021). Again, numerical simulations have confirmed the direct correspondence between the fractional helicity of magnetic fields and the resulting circular polarization of GWs (Kahniashvili et al 2021).…”

Section: Introductionmentioning

confidence: 90%

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Simulating relic gravitational waves from inflationary magnetogenesis

Brandenburg,

Sharma

2021

Preprint

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We present three-dimensional direct numerical simulations of the production of magnetic fields and gravitational waves (GWs) in the early Universe during a low energy scale matter-dominated postinflationary reheating era, and during the early subsequent radiative era, which is strongly turbulent. The parameters of the model are determined such that it avoids a number of known physical problems and produces magnetic energy densities between 0.2% and 2% of the critical energy density at the end of reheating. During the subsequent development of a turbulent magnetohydrodynamic cascade, magnetic fields and GWs develop a spectrum that extends to higher frequencies in the millihertz (nanohertz) range for models with reheating temperatures of around 100 GeV (150 MeV) at the beginning of the radiation-dominated era. However, even though the turbulent cascade is fully developed, the GW spectrum shows a sharp drop for frequencies above the peak value. This suggests that the turbulence is less efficient in driving GWs than previously thought. The peaks of the resulting GW spectra may well be in the range accessible to space interferometers, pulsar timing arrays, and other facilities.

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“…Several physical situations which may cause the Schwinger effect are discussed, such as relativistic heavy ion collisions [6], neutron stars [7,8], charged black holes [9,10], and inflation with the amplification of the electromagnetic fields [11][12][13][14][15][16][17][18][19][20][21][22][23][24]. In particular, such inflation models are intensively studied in the context of magnetogenesis and baryogenesis.…”

Section: Introductionmentioning

confidence: 99%

When does the Schwinger Preheating Occur?

Okano,

Fujita

2021

Preprint

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When the inflaton couples to photons and amplifies electric fields, charged particles produced via the Schwinger effect can dominate the universe after inflation, which is dubbed as the Schwinger preheating. Using the hydrodynamic approach for the Boltzmann equation, we numerically study two cases, the Starobinsky inflation model with the kinetic coupling and the anisotropic inflation model. The Schwinger preheating is not observed in the latter model but occurs for a sufficiently large inflaton-photon coupling in the first model. We analytically address its condition and derive a general attractor solution of the electric fields. The occurrence of the Schwinger preheating in the first model is determined by whether the electric fields enter the attractor solution during inflation or not.

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Chiral gravitational waves produced in a helical magnetogenesis model

Cited by 22 publications

References 86 publications

Analytic study of dark photon and gravitational wave production from axion

Analytic study of dark photon and gravitational wave production from axion

Simulating relic gravitational waves from inflationary magnetogenesis

When does the Schwinger Preheating Occur?

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